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u‰‰ID u‰‰ŽÒ–¼ Š‘®‘åŠw Šw”N u‰‰ƒ^ƒCƒgƒ‹
µ‘Òu‰‰ ìŸ –] Ž ’}”g‘åŠw ‹â‰Í’†S‚Éö‚Þ’´‹‘åƒuƒ‰ƒbƒNƒz[ƒ‹Œ`¬‚Í‚Ç‚±‚Ü‚Å•ª‚©‚Á‚½‚Ì‚©H
µ‘Òu‰‰ “c‘º —zˆê Ž ‘—§“V•¶‘ä ƒTƒuƒ~ƒŠ”g[‰F’ˆ’T¸‚Ì‚¢‚ÜE–¢—ˆ
µ‘Òu‰‰ “¡“c —T Ž ‘åã‘åŠw ‚ƒGƒlƒ‹ƒM[“V‘Ì‚Æ‚µ‚Ä‚Ì‹â‰Í’c
‹â‰Í01a Αq –¢“Þ –kŠC“¹‘åŠw M1 Formation of z`6 Quasars from Hierarchical Galaxy Mergers
‹â‰Í02a ’r“c _”V ˆ¤•Q‘åŠw M2 COSMOS“Vˆæ‚É‚¨‚¯‚é’áŒõ“xƒNƒF[ƒT[’T¸
‹â‰Í03a Žsì K•½ ‹ž“s‘åŠw M1 ’´‚Œõ“xÔŠOü‹â‰ÍULIRG‚̃Gƒlƒ‹ƒM[Œ¹f’f–@
‹â‰Í04b M“c ˜aÆ “Œ–k‘åŠw M1 ‚·‚΂é‚̃XƒyƒNƒgƒ‹ƒf[ƒ^‚ð—p‚¢‚½AGN‚ÌŽ¿—ʂƃGƒfƒBƒ“ƒgƒ“”ä‚ÉŠÖ‚·‚錤‹†
‹â‰Í05b ãù ®Æ ˆ¤•Q‘åŠw M1 XMM-Newton‚ð—p‚¢‚½Xü‹­“x•Ï“®‚ªŒƒ‚µ‚¢Šˆ“®‹â‰ÍŠj‚Ì’Tõ
‹â‰Í06c Îè „Žj ‘‡Œ¤‹†‘åŠw‰@‘åŠw M2 Search for High-z Quasars beyond z=6.5 with Subaru Telescope
‹â‰Í07c ‘O—Ñ —²”V “Œ–k‘åŠw M2 Šˆ“®‹â‰ÍŠj‚ÌŠˆ“®«‚Æ•ê‹â‰ÍŠÂ‹«‚ɂ‚¢‚Ä
‹â‰Í08b r–Ø é—Y ˆ¤•Q‘åŠw M1 ‚·‚΂é–]‰“‹¾‚ÌMOIRCS‚ð—p‚¢‚Ä“¾‚½N-loud QSO‚ÌÃŽ~Œn‰ÂŽ‹ƒXƒyƒNƒgƒ‹‚̉ðÍ
‹â‰Í09c ¼‰ª Œ’‘¾ ˆ¤•Q‘åŠw D1 ’‚‘f‹Pü‚©‚ç’T‚銈“®‹â‰ÍŠj‚ƯŒ`¬Šˆ“®‚ÌŠÖŒW
‹â‰Í10b —Ñ —²”V “Œ‹ž‘åŠw M2 VLBI‚Å’T‚éƒNƒF[ƒT[L‹zŽûü‚Ì‹NŒ¹
‹â‰Í11a ŽÂ–Ø VŒá “Œ‹ž‘åŠw M1 ‰“•û‚Æ‹ß–T‚̯Œ`¬‹â‰Í‚ÌŒ`‘Ô”äŠr
‹â‰Í12a ‹´–{ ‘ñ–ç “Œ‹ž‘åŠw M1 The Properties of Lyman ƒ¿ emitters (LAEs)
‹â‰Í13b ”n“n Œ’ “Œ–k‘åŠw M1 Ly ƒ¿‹Pü‹â‰ÍŠÏ‘ª‚̈Ӌ`‚Æ‚–§“x—̈æ53W002‚ÌŒ¤‹†
‹â‰Í14c ¬–ì ‹Xº “Œ‹ž‘åŠw D2 Stellar Populations of Lyman Alpha Emitters at z`6-7
‹â‰Í15c —é–Ø Œ«‘¾ “Œ‹ž‘åŠw D1 z=2.48‚Ì“d”g‹â‰Í4C 23.56—̈æ‚É‚¨‚¯‚鯌`¬‹â‰Í‚ÆŒ´Žn‹â‰Í’c‚ÌŒ`¬
‹â‰Í16b Š™“c ”ü ˆ¤•Q‘åŠw M1 COSMOS“Vˆæ‚É‚¨‚¯‚郉ƒCƒ}ƒ“ƒuƒŒ[ƒN‹â‰ÍiLBGj‚̃TƒCƒYi‰»
‹â‰Í17b —Ñ q•½ “Œ–k‘åŠw M1 ƒ~ƒbƒVƒ“ƒOƒTƒeƒ‰ƒCƒg–â‘è‚ÌÄ’è‹`‚Æá⬋â‰Í‚̯Œ`¬—}§‰ß’ö‚©‚猩‚½–â‘è‰ðŒˆ‚ɂ‚¢‚Ä
‹â‰Í18a ”~”¨ ‹‹I “Œ‹ž‘åŠw M1 Diffuse interstellar PAH emission in the LMC observed with the AKARI/IRC
‹â‰Í19a ’·‰® •¶Žq –¼ŒÃ‰®‘åŠw M1 ‹â‰Íi‰»‚©‚猩‚½ƒ_ƒXƒgŒ¸Œõ‚Ì”•¨——ʂւ̈ˑ¶«‚ÌŒ¤‹†
‹â‰Í20a ŠÚ“à Œª “Œ‹ž‘åŠw M1 miniTAO–]‰“‹¾‹ßÔŠOƒJƒƒ‰ANIR‚É‚æ‚é‹ß–TLIRGs‚ÌPa ƒ¿ŠÏ‘ª
‹â‰Í21a ŽR‰º ‘ñŽž “Œ‹žH‹Æ‘åŠw M1 –ì•ÓŽR45m‚ð—p‚¢‚½LIRGs‚Ì12CO(J=1-0)ƒT[ƒxƒCŠÏ‘ª
‹â‰Í22a ŽOàV —Ú‰Ô “Œ‹žŠwŒ|‘åŠw M2 á⬕s‹K‘¥‹â‰ÍNGC4449‚Ì’ªŽ¬”ö‚É‚¨‚¯‚鯌`¬
‹â‰Í23c •S£ 仌bŽq “Œ‹ž‘åŠw D2 Star formation efficiency in the Barred Spiral Galaxy NGC 4303
‹â‰Í24b âˆä Ls Ž­Ž™“‡‘åŠw M2 VERA‚É‚æ‚é‹â‰ÍŒnŠO‰•”‰ñ“]‹ÈüIFIRAS 05168+3634‚Ì”NŽüŽ‹·‘ª’è
‹â‰Í25b —é–Ø –L Ž­Ž™“‡‘åŠw M2 ‹â‰ÍŒnŠO‰•”OBŒ^Œó•â¯‚Ì•ªŒõ’ÇŠÏ‘ª
‹â‰Í26b ’†‘º ãÄ “Œ–k‘åŠw M1 Ž¥‹C—¬‘̃Vƒ~ƒ…ƒŒ[ƒVƒ‡ƒ“‚Æ3ŽŸŒ³‚Ì‘å‹Ç“I‹â‰ÍŽ¥ê\‘¢‚ÌŒ¤‹†
‹â‰Í27a ’†”ö Œõ –kŠC“¹‘åŠw M1 Determining Star Formation Timescale and Pattern Speed in Nearby Spiral Galaxies
‹â‰Í28a ŽáŽR ^—œŽq –kŠC“¹‘åŠw M1 ‹â‰Í‰~”Õ‚Í‹â‰Í‡‘Ì‚ð‚Ç‚¤Ø‚蔲‚¯‚Ķ‚«Žc‚é‚©
‹â‰Í29c Š}ˆä ˜i “Œ–k‘åŠw M1 ‰~”Õ‹â‰Í“¯Žm‚̇‘̃Vƒ~ƒ…ƒŒ[ƒVƒ‡ƒ“
‹â‰Í30a ‹e’r ‘å•ã ç—t‘åŠw M1 ‹â‰ÍÕŒ‚”g‚É”º‚¤Wiggle Instability‚ÌÄŒŸ“¢
‹â‰Í31a •ž•” Œö•½ “Œ‹ž‘åŠw M2 ‹â‰ÍŒnƒnƒ[‚̯‚Ì‹O“¹—£S—¦•ª•z‚©‚ç’T‚é‹â‰ÍŒnŒ`¬Žj
‹â‰Í32a Sengul Ozden “Œ‹ž‘åŠw M1 Search for plasma heating mechanisms in non-cD clusters
‹â‰Í33a ²‹vŠÔ ŠG— “Œ‹ž—‰È‘åŠw M1 Xü“V•¶‰q¯u‚·‚´‚­v‚É‚æ‚éƒPƒ“ƒ^ƒEƒ‹ƒXÀ‹â‰Í’c‚ÌdŒ³‘f•ª•z‚ÌŒˆ’è
‹â‰Í34a —˜ì ‘‡Œ¤‹†‘åŠw‰@‘åŠw M1 SDF“Vˆæ‚É‚¨‚¯‚éz`6‚ÌŒ´Žn‹â‰Í’c‚Ì’T¸
‹â‰Í35a “c’† Œ« ’}”g‘åŠw M1 GPU‚ð—p‚¢‚½“V‘Ì•¨—ƒVƒ~ƒ…ƒŒ[ƒVƒ‡ƒ“

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